Radio detection of cosmic radiation Janusz Zabierowski Narodowe Centrum Badań Jądrowych
Astrofizyka Cząstek w Polsce – Kraków-Przegorzały, 3-6.03.2013
Content
Why radio detection of EAS is so attractive;
Some history of the research;
What we have already learned about radio emission of EAS;
Overview of the main experiments in MHz band;
EAS observations using microwave radiation;
Radio in solids – search for UHE neutrinos.
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Aims of radio detection (B. Revenu, ARENA 2012, Erlangen Germany)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Aims of radio detection (B. Revenu, ARENA 2012, Erlangen Germany)
And then (only then), we will answer to the FAQ: What about a huge radio array over tens or thousends of km2? J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Advantages of Radio Emission from Air Showers (I)
Scintillators measure only electrons (or muons) left in the shower.
These numbers depend sensitively on shower maximum. This, in turn, depends on primary particle composition.
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Advantages of Radio Emission from Air Showers (I)
Scintillators measure only electrons (or muons) left in the shower.
These numbers depend sensitively on shower maximum. This, in turn, depends on primary particle composition.
Radio signal is created by all electrons - we have bolometric measurement (integral over shower evolution), hence: Radio signal gives energy; Polarisation measurements provide extra information.
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Advantages of Radio Emission from Air Showers (II)
Radio has an advantage in hybrid observations (e.g. scintillator + fluorescence):
same duty cycle as scintillators (minus only thunderstorms) what may increase hybrid event rate by factor of ten if co-located with AUGER. (H.Falcke, LOPES Day 2007)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Advantages of Radio Emission from Air Showers (III)
Mostly coherent processes, radio power increases quadratically with energy;
(H.Falcke, LOPES Day 2007)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Advantages of Radio Emission from Air Showers (III)
Mostly coherent processes, radio power increases quadratically with energy;
Low attenuation in atmosphere and
dielectric solids (can see also distant and inclined showers);
(H.Falcke, LOPES Day 2007)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Advantages of Radio Emission from Air Showers (III)
Mostly coherent processes, radio power increases quadratically with energy;
Low attenuation in atmosphere and
dielectric solids (can see also distant and inclined showers);
Cheap detectors, easy to deploy;
(H.Falcke, LOPES Day 2007)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Advantages of Radio Emission from Air Showers (III)
Mostly coherent processes, radio power increases quadratically with energy;
Low attenuation in atmosphere and
dielectric solids (can see also distant and inclined showers);
Cheap detectors, easy to deploy; A promising tool for the detection of UHE neutrinos (in ice, salt or lunar regolith);
(H.Falcke, LOPES Day 2007)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Advantages of Radio Emission from Air Showers (III)
Mostly coherent processes, radio power increases quadratically with energy;
Low attenuation in atmosphere and
dielectric solids (can see also distant and inclined showers);
Cheap detectors, easy to deploy; A promising tool for the detection of UHE neutrinos (in ice, salt or lunar regolith); Potential problems: Radio freq. interference (RFI); correlation with other parameters – still under investigation; only practical above ~1017 eV.
(H.Falcke, LOPES Day 2007)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Early history of EAS radio theory and experiments (I)
Jelley: considered existence of radio Čerenkov emission from EAS
Kahn & Lerche: geomagnetically induced transverse currents
Askaryan: coherent charge excess variation
Allan Colgate
Fuji & Nishimura
Castagnoli et al.
1958 1959 1960 1961 1962 1963 1964 1965 1966 1967 1968 1969
Jelley et al.: experimental detection J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Early history of EAS radio theory and experiments (I)
Jelley: considered existence of radio Čerenkov emission from EAS
Kahn & Lerche: geomagnetically induced transverse currents
Askaryan: coherent charge excess variation
Allan Colgate
Fuji & Nishimura
Harwell, Jordell Bank and Dublin team found pulses Castagnoli et al. at 44MHz, establishing beyond doubt that showers can emit detectable pulses 1958 1959 1960of electromagnetic 1961 1962 1963 1964 1965 1966 1967 1968 1969 radiation. Jelley al. Nature 205 (1965)detection Jelley etatal.: experimental J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Early history of EAS radio theory and experiments (I)
Jelley: considered existence of radio Čerenkov emission from EAS
Kahn & Lerche: geomagnetically induced transverse currents
Askaryan: coherent charge excess variation
Allan Colgate
Fuji & Nishimura
Castagnoli et al.
1958 1959 1960 1961 1962 1963 1964 1965 1966 1967 1968 1969
Jelley et al.: experimental detection J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Early history of EAS radio theory and experiments (II)
Stimulated by the theoretical works there was large experimental activity around the world in the late 60ies & early 70ies of the 20th century. Emission from 2 MHz up to 520 MHz was found.
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Early history of EAS radio theory and experiments (II)
Stimulated by the theoretical works there was large experimental activity around the world in the late 60ies & early 70ies of the 20th century. Emission from 2 MHz up to 520 MHz was found. In the mid 70ies air-shower radio detection activities ceased almost completely due to: difficulty with radio interference, uncertainty about the interpretation of experimental results, restrictions of analog data processing. Moreover radio astronomers moved to GHz region and other air-shower detection techniques had considerable success.
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Early history of EAS radio theory and experiments (III)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Revival just after 2000 Revival of the theoretical and experimental activity started with LOPES and CODALEMA experiments in 2003. ¾ Exploration of the
decameter region (30 MHz) by astronomers
¾ Digital electronics instead of analog; ¾ Computing techniques (beam forming, filtering)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Cosmic Rays Radio Detection Revival
RADHEP-2000 First International Workshop on Radio Detection of High-Energy Particles UCLA Faculty Center University of California, Los Angeles November 16-18, 2000
52 participants, 31 talks
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Cosmic Rays Radio Detection Revival
RADHEP-2000 First International Workshop on Radio Detection of High-Energy Particles UCLA Faculty Center University of California, Los Angeles November 16-18, 2000
52 participants, 31 talks „No „golden signal” seen for an RF transient associated with EAS of cosmic rays at CASA.” – - J. Rosner (Univ of Chicago)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Cosmic Rays Radio Detection Revival January 2004: First detection of CR radio pulse by LOPES (H. Falcke et al. Nature 435 (2005) 313 ) Confirmed by CODALEMA at Nançay (D. Ardouin et al.. NIM A555 (2005) )
RADHEP-2000 First International Workshop on Radio Detection of High-Energy Particles UCLA Faculty Center University of California, Los Angeles November 16-18, 2000
52 participants, 31 talks „No „golden signal” seen for an RF transient associated with EAS of cosmic rays at CASA.” – - J. Rosner (Univ of Chicago)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Cosmic Rays Radio Detection Revival January 2004: First detection of CR radio pulse by LOPES (H. Falcke et al. Nature 435 (2005) 313 ) Confirmed by CODALEMA at Nançay (D. Ardouin et al.. NIM A555 (2005) )
RADHEP-2000
First International Workshop on Radio Detection of High-Energy Particles
UCLA Faculty Center University of California, Los Angeles November 16-18, 2000
52 participants, 31 talks „No „golden signal” seen for an RF transient associated with EAS of cosmic rays at CASA.” – - J. Rosner (Univ of Chicago)
Strong coherent radio pulse coincident with air shower First ever all-sky radio-only mapping Imaging (AZ-EL) with time resolution of 12.5 ns Total duration is ~200 ns No cleaning was performed, side lobes still visible Location of burst agrees with KASCADE location to within 0.5°.
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Cosmic Rays Radio Detection Revival January 2004: First detection of CR radio pulse by LOPES (H. Falcke et al. Nature 435 (2005) 313 ) Confirmed by CODALEMA at Nançay (D. Ardouin et al.. NIM A555 (2005) )
RADHEP-2000
First International Workshop on Radio Detection of High-Energy Particles
UCLA Faculty Center University of California, Los Angeles November 16-18, 2000
52 participants, 31 talks „No „golden signal” seen for an RF transient associated with EAS of cosmic rays at CASA.” – - J. Rosner (Univ of Chicago)
Strong coherent radio pulse coincident with air shower First ever all-sky radio-only mapping Imaging (AZ-EL) with time resolution of 12.5 ns Total duration is ~200 ns No cleaning was performed, side lobes still visible Location of burst agrees with KASCADE location to within 0.5°. First detection of Cosmic Ray radio pulse in “modern times”, with highest temporal and spatial resolution ever achieved.
¾
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Current understanding of radio emission from air showers – physical processes (I) Coherent emission processes: - predominantly of geomagnetic origin - typical frequencies: several tens of MHz - emission in forward direction ¾ confirmed with LOPES and CODALEMA Current experimental results are compatible with contributions from all mechanisms as long as geomagnetic is dominant
(F. Schroeder – ARENA2012)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Current understanding of radio emission from air showers – physical processes (I) Coherent emission processes: - predominantly of geomagnetic origin - typical frequencies: several tens of MHz - emission in forward direction ¾ confirmed with LOPES and CODALEMA Current experimental results are compatible with contributions from all mechanisms as long as geomagnetic is dominant
1. Geomagnetic deflection of e- and e+ results in transient currents - dominant effect (Kahn, Lerche 1966) ¾ confirmed with LOPES (and others) (F. Schroeder – ARENA2012)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Current understanding of radio emission from air showers – physical processes (I) Coherent emission processes: - predominantly of geomagnetic origin - typical frequencies: several tens of MHz - emission in forward direction ¾ confirmed with LOPES and CODALEMA Current experimental results are compatible with contributions from all mechanisms as long as geomagnetic is dominant
1. Geomagnetic deflection of e- and e+ results in transient currents - dominant effect (Kahn, Lerche 1966) ¾ confirmed with LOPES (and others)
2. Variation of the dipole strength of the shower
(F. Schroeder – ARENA2012)
shower = emitting dipole antenna (smaller effect) J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Current understanding of radio emission from air showers – physical processes (II) 3. Askaryan effect (varying net charge) - ~10 times weaker than geomagnetic effect ¾ Strong indications by CODALEMA and AERA
F. Schroeder – ARENA2012
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Current understanding of radio emission from air showers – physical processes (II) 3. Askaryan effect (varying net charge) - ~10 times weaker than geomagnetic effect ¾ Strong indications by CODALEMA and AERA 4. Cherenkov emission in radio frequencies – - also referred as Askaryan emission (being easily confound and not well separated from net charge variation); ¾ important for particle showers in dense media (n>1) ¾ not clear whether negligible against Askaryan; ¾ until now, only for accelerator beam induced showers radio emission in dense media was observed.
F. Schroeder – ARENA2012
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Current understanding of radio emission from air showers – physical processes (III) 5. Geosynchrotron (Falcke, Goram 2003) - part of geomagnetic emission ¾ essential or small sub-effect?
F. Schroeder – ARENA2012
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Current understanding of radio emission from air showers – physical processes (III) 5. Geosynchrotron (Falcke, Goram 2003) - part of geomagnetic emission ¾ essential or small sub-effect? 6. Atmospheric electric fields - strong effect during thunderstorms, but not during normal weather; ¾ duty-cycle reduced by < 5 %.
F. Schroeder – ARENA2012
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Current understanding of radio emission from air showers – physical processes (III) 5. Geosynchrotron (Falcke, Goram 2003) - part of geomagnetic emission ¾ essential or small sub-effect? 6. Atmospheric electric fields - strong effect during thunderstorms, but not during normal weather; ¾ duty-cycle reduced by < 5 %.
7. Molecular bremsstrahlung – under investigation; ¾ partly coherent GHz emission from weakly ionised shower plasmas observed in accelerator beam measurements ¾ isotropic emission – technique with advantage for shower detection at large lateral distances.
F. Schroeder – ARENA2012
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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First order: geomagnetic emission
time-varying transverse currents
signal strength ~ v x B = v B sin(α)
purely linear polarisation
E-field vector aligned with v x B for all observer locations
emission can be „compressed“ by Cherenkov effects
diagrams by K.D. de Vries
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Second order: Askaryan emission
Askaryan: time-varying chargeexcess also occurs for n=1! Cherenkov effects „compress“ the emission not „classical“ Cherenkov emission of a non-varying net charge linearly polarized E-field vector radially oriented, varies with observer location relative to core
diagrams by K.D. de Vries
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Askaryan effect: experimental indications
(F. Schroeder, LOPES-Meeting 24.10.2012, Freudenstadt)
Geomagnetic + Askaryan included in calculations
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Modern radio experiments (I)
LOPES
(= LOFAR PrototypE Station)
- digital radio interferometer at KIT, Germany, co-located with KASCADE-Grande - proof of the principle experiment (Nature, 2005)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Modern radio experiments (I)
LOPES
(= LOFAR PrototypE Station)
- digital radio interferometer at KIT, Germany, co-located with KASCADE-Grande - proof of the principle experiment (Nature, 2005)
LOFAR - digital low frequency interferometer for radio astronomy,
Nederlands and other European countries. - Detection of cosmic air showers and neutrino induced particle showers in the lunar regolith – one of Key Science Projects.
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Modern radio experiments (I)
LOPES
(= LOFAR PrototypE Station)
- digital radio interferometer at KIT, Germany, co-located with KASCADE-Grande - proof of the principle experiment (Nature, 2005)
LOFAR - digital low frequency interferometer for radio astronomy,
Nederlands and other European countries. - Detection of cosmic air showers and neutrino induced particle showers in the lunar regolith – one of Key Science Projects.
CODALEMA – at the decametric radio observatory of Nançay, France
Advantage: radio quiet environment Disadvantage: relatively simple scintillator EAS array for shower detection
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Modern radio experiments (I)
LOPES
(= LOFAR PrototypE Station)
- digital radio interferometer at KIT, Germany, co-located with KASCADE-Grande - proof of the principle experiment (Nature, 2005)
LOFAR - digital low frequency interferometer for radio astronomy,
Nederlands and other European countries. - Detection of cosmic air showers and neutrino induced particle showers in the lunar regolith – one of Key Science Projects.
CODALEMA – at the decametric radio observatory of Nançay, France
Advantage: radio quiet environment Disadvantage: relatively simple scintillator EAS array for shower detection
Most of the progress in the field of digital radio detection in recent years was either made by LOPES or CODALEMA J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Modern radio experiments (II)
AERA
(= Auger Engineering Radio Array)
- next generation digital radio array under construction at PAO, Argentina Investigation of the performance of radio technique by cross-calibration with surface particle detectors and fluorescence light detectors
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Modern radio experiments (II)
AERA
(= Auger Engineering Radio Array)
- next generation digital radio array under construction at PAO, Argentina Investigation of the performance of radio technique by cross-calibration with surface particle detectors and fluorescence light detectors
Tunka-Rex – EAS array of air-Cherenkov detectors, by Irkutsk, Russia - currently, a new hybrid approach investigated with several radio prototype setups
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Modern radio experiments (II)
AERA
(= Auger Engineering Radio Array)
- next generation digital radio array under construction at PAO, Argentina Investigation of the performance of radio technique by cross-calibration with surface particle detectors and fluorescence light detectors
Tunka-Rex – EAS array of air-Cherenkov detectors, by Irkutsk, Russia - currently, a new hybrid approach investigated with several radio prototype setups
CROME (= Cosmic-Ray Observatorium via Microwave Emission) - located in the center of KASCADE-Grande array, KIT, Germany. Test beam measurement by Gorham et al.(PRD 2008) has found non-coherent, unpolarized, isotropic, 10 ns life-time, 1-6 GHz molecular brehmsstrahlung emission by ~10 eV electrons.
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Modern radio experiments (II)
AERA
(= Auger Engineering Radio Array)
- next generation digital radio array under construction at PAO, Argentina Investigation of the performance of radio technique by cross-calibration with surface particle detectors and fluorescence light detectors
Tunka-Rex – EAS array of air-Cherenkov detectors, by Irkutsk, Russia - currently, a new hybrid approach investigated with several radio prototype setups
CROME (= Cosmic-Ray Observatorium via Microwave Emission) - located in the center of KASCADE-Grande array, KIT, Germany. Test beam measurement by Gorham et al.(PRD 2008) has found non-coherent, unpolarized, isotropic, 10 ns life-time, 1-6 GHz molecular brehmsstrahlung emission by ~10 eV electrons. Finding such a signal from EAS will provide low-cost detector with 100% duty-cycle, giving calorimetric measurement of longitudinal shower development. J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Modern radio experiments – - oriented on neutrino search (III)
Radio at IceCube and IceTop – at South Pole
Plans to extend IceTop with radio antennas radio measurement of longitudinal shower development can improve the reconstruction accuracy of IceTop; antennas cover larger area than IceTop and can provide an additional veto for IceCube, even for more inclined showers;
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Modern radio experiments – - oriented on neutrino search (III)
Radio at IceCube and IceTop – at South Pole
Plans to extend IceTop with radio antennas radio measurement of longitudinal shower development can improve the reconstruction accuracy of IceTop; antennas cover larger area than IceTop and can provide an additional veto for IceCube, even for more inclined showers;
ARA (= Askaryan Radio Array) – at South Pole – planned to investigate in-ice radio detection of neutrino showers.
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Modern radio experiments – - oriented on neutrino search (III)
Radio at IceCube and IceTop – at South Pole
Plans to extend IceTop with radio antennas radio measurement of longitudinal shower development can improve the reconstruction accuracy of IceTop; antennas cover larger area than IceTop and can provide an additional veto for IceCube, even for more inclined showers;
ARA (= Askaryan Radio Array) – at South Pole – planned to investigate in-ice radio detection of neutrino showers.
ANITA (= Antarctic Impulsive Transient Antenna) – baloon borne
radio interferometer for neutrino detection with Askaryan emission from ice no neutrino observation yet (candidates only); claims of succesful detection of geomagnetic radio pulses at energies ~1019 eV (reflected from ice) – questiond because at 300 - 1000 MHz models do not predict coherent geomagnetic emission J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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LOPES (LOfar PrototypE Station) 2003 - 2012
30 dipole antennas (40 – 80 MHz) in different polarisation configurations at well calibrated air-shower experiment KASCADE-Grande
Goals:
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LOPES history
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Digital radio interferometry
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Energy reconstruction
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Lateral distribution: LOPES vs. simulation
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Energy and Xmax sensitivity of radio emission- theoretical prediction energy determination at distance with minimum fluctuations Xmax determination from lateral slope Fe – flat p – steeper, fluctuating g – steepest, fluctuating
original investigation for REAS2, but same qualitative behaviour for REAS3, MGMR, Konstantinov et al. Huege, Ulrich, Engel (Astrop. Phys. 2008)
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Energy and Xmax sensitivity
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Correlation with Muon Tracking Detector
r= - 0.44±0.12
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Conclusions from LOPES
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Epoch of Reionisation Deep extragalactic surveys Transient sources Ultra high energy cosmic rays Solar science and space weather Cosmic magnetism
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circle size corresponds to signal strength
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Conclusions: LOFAR ¾ LOFAR is steadily taking data, having currently detected > 160 cosmic ray events of good quality; ¾ LOFAR has the highest density of antennas of any air shower experiment for radio detection; ¾ LOFAR team has demonstrated a capability to make in the future this radiotelescope a useful device for UHE CR research
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The CODALEMA collaboration 8 French laboratories 1 experimental site at Nançay (Observatoire de Paris)
Observatory Paris‐Meudon LAL Orsay ESEO Angers Subatech Nantes
Radio Telescope O.Ravel – ARENA 2010, Nantes, France
LPCE Orléans
Observatoire de Nançay
COsmic ray Detection Array with Logarithmic Electro Magnetic Antennas
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LAOB Besançon
LPSC Grenoble
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CODALEMA : stage I
2002-2005
Revival of the cosmic ray radio detection method in 2002 with the CODALEMA and LOPES experiments. Nançay Decametric Array (DAM)
8 bit 1Gs/s)
TRIGGER: 4 Stations of Scintillators (2 m2) in time coincidences Signal recording + Time of flight analysis Conical log-periodic antenna Frequency bandwidth : 1-100 MHz
O.Ravel – ARENA 2010, Nantes, France
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CODALEMA 2 : 2006 – 2011 (0.25 km2) Antenna array in the slave mode of the scintillator array
3 detector arrays: Antenna array 21 dipoles oriented EW 3 dipoles oriented NS Analyses 24 – 82 MHz
Decametric array Scintillator array:
18 groups of 8 Phased logperiodic antennas Electric field map at small scale
P.Lautridou, ARENA 2012, Erlangen, Germany
O.Ravel – ARENA 2010, Nantes, France
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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CODALEMA 3: 2011…@ Nançay
Self-triggered antennas +multiscale array (=> 1 km2) Design validated at Pierre Auger Laboratory
P.Lautridou, ARENA 2012, Erlangen, Germany
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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CODALEMA 2: emission mechanisms - experimental proofs
(D.T. Machado, ECRS 2012, Moscow, Russia)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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CODALEMA 2: emission mechanisms - experimental proofs
(D.T. Machado, ECRS 2012, Moscow, Russia)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Radio@Pierre Auger Observatory - based on LOPES and CODALEMA experience
M. Melissas – ARENA 2012, Erlangen, Germany
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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AMIGA
M. Melissas – ARENA 2012, Erlangen, Germany
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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AERA Goals 1. Develop new instrumental technique for EAS radio detection in the MHz. 2. Study the feasibility of large scale radio detection at the Pierre Auger Observatory. 3. Cosmic ray physics in the transition region
M. Melissas – ARENA 2012, Erlangen, Germany
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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M. Melissas – ARENA 2012, Erlangen, Germany
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Tunka-Rex
Planned setup
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Air shower observation using Microwave Radiation Introduction to Molecular Brehmsstrahlung by Ralph Engel (ARENA 2012, Erlangen, Germany)
Motivation: In accelerator experiment a broadband microwave emission from air ionized via high-energy electrons and photons was observed.
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Air shower observation using Microwave Radiation Introduction to Molecular Brehmsstrahlung by Ralph Engel (ARENA 2012, Erlangen, Germany)
Motivation: In accelerator experiment a broadband microwave emission from air ionized via high-energy electrons and photons was observed.
If found in EAS the microwave detection will be a high-duty cycle complement to current nitrogen fluorecsence observations. J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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(R.Engel – ARENA 2012, Erlangen, Germany)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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(R.Engel – ARENA 2012, Erlangen, Germany)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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(R.Engel – ARENA 2012, Erlangen, Germany)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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(R.Engel – ARENA 2012, Erlangen, Germany)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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P. Facal San Luis – ARENA 2012
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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(R.Engel – ARENA 2012, Erlangen, Germany)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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(Air-shower Microwave Bremsstrahlung Experimental Radiometer)
(R.Engel – ARENA 2012, Erlangen, Germany)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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(R.Engel – ARENA 2012, Erlangen, Germany)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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(R.Engel – ARENA 2012, Erlangen, Germany)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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KASCADE-Grande reconstruction uncertainties: 0.8o - arrival direction 6 m - core position 20% - energy
(R.Engel – ARENA 2012, Erlangen, Germany)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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CROME Group
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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(R.Smida – ARENA 2012, Erlangen, Germany)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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GHz radio emission from air showers?
EASIER in Auger CROME Cherenkov-boosted air shower radio emission?
R. Smida, UHECR2012 workshop J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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(R.Engel – ARENA 2012, Erlangen, Germany)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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At conference UHECR 2012 (CERN, Feb 2012) two experiments, EASIER (Auger) and CROME announced the first measurements of microwave signal from air showers in the C band (3.4 – 4.2 GHz)
(R.Engel – ARENA 2012, Erlangen, Germany)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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(R.Engel – ARENA 2012, Erlangen, Germany)
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Radio in solids
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Ultra High-energy (super GZK) neutrino detection from Moon
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Radio observation of Moon: different frequencies
H. Falcke – RadioDetection – 2007-06-17 –Charlottesville-Future
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Radio telescope observations of Moon - UHE neutrinos and cosmic rays at E >1020 eV
LORD
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Summary – Radio in solids New technique after idea in the 60’s
- relatively easy, but …. still a lot of R&D is required - potencial for huge volumes - THE tool for the highest energies (E » EGZK) Lots of activities, experimental, theoretical, technological and
observational
Proof of principle is done only in the laboratory, next step has to be to find a UHE neutrino at all.
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Podsumowanie ogólne Miniona dekada jest świadkiem intensywnego rozwoju tej metody
badawczej, tak w aspekcie teoretycznym jak eksperymentalnym; czynne zaangażowanie polskich naukowców (LOPES, CROME, AERA), które należałoby kontynuować (AERA, LOFAR?);
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Podsumowanie ogólne Miniona dekada jest świadkiem intensywnego rozwoju tej metody
badawczej, tak w aspekcie teoretycznym jak eksperymentalnym; czynne zaangażowanie polskich naukowców (LOPES, CROME, AERA), które należałoby kontynuować (AERA, LOFAR?); Coraz lepsze wyniki w wyznaczaniu parametrów wielkich
pęków w oparciu o mierzone sygnały radiowe napawają optymizmem, choć jeszcze potrzeba wiele pracy;
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Podsumowanie ogólne Miniona dekada jest świadkiem intensywnego rozwoju tej metody
badawczej, tak w aspekcie teoretycznym jak eksperymentalnym; czynne zaangażowanie polskich naukowców (LOPES, CROME, AERA), które należałoby kontynuować (AERA, LOFAR?); Coraz lepsze wyniki w wyznaczaniu parametrów wielkich
pęków w oparciu o mierzone sygnały radiowe napawają optymizmem, choć jeszcze potrzeba wiele pracy;
Hybrydowe pomiary wielkich pęków z zastosowaniem anten w
aparaturach liczących dziesiątki tysięcy km2 coraz bardziej realne.
J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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Podsumowanie ogólne Miniona dekada jest świadkiem intensywnego rozwoju tej metody
badawczej, tak w aspekcie teoretycznym jak eksperymentalnym; czynne zaangażowanie polskich naukowców (LOPES, CROME, AERA), które należałoby kontynuować (AERA, LOFAR?); Coraz lepsze wyniki w wyznaczaniu parametrów wielkich
pęków w oparciu o mierzone sygnały radiowe napawają optymizmem, choć jeszcze potrzeba wiele pracy;
Hybrydowe pomiary wielkich pęków z zastosowaniem anten w
aparaturach liczących dziesiątki tysięcy km2 coraz bardziej realne.
Ambitny cel : Radiodetekcja lepsza od technik konwencjonalnych!? J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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J. Zabierowski - Astrofizyka Cząstek w Polsce - Kraków-Przegorzały 3-6. 03. 2013 r.
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